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Global resurfacing of Uranus's moon Miranda by convection

Noah P. Hammond and Amy C. Barr
Global resurfacing of Uranus's moon Miranda by convection
Geology (Boulder) (November 2014) 42 (11): 931-934


Miranda, an icy moon of Uranus, is one of the most visually striking and enigmatic bodies in the solar system. Three polygonal-shaped regions of intense deformation, dubbed "coronae," dominate the surface of Miranda. Here we use numerical methods to show that sluggish-lid convection in Miranda's ice shell, powered by tidal heating, can simultaneously match the global distribution of coronae, the concentric deformation pattern, and the estimated heat flow during formation. The expected rheological conditions in Miranda's ice shell lead to the development of low-order convection that produces surface deformation patterns similar to those observed. We find that satellite core size strongly controls convection geometry and that low-order convection patterns are much more stable for core radii less than half the satellite radius.

ISSN: 0091-7613
EISSN: 1943-2682
Serial Title: Geology (Boulder)
Serial Volume: 42
Serial Issue: 11
Title: Global resurfacing of Uranus's moon Miranda by convection
Affiliation: Brown University, Department of Geological Sciences, Providence, RI, United States
Pages: 931-934
Published: 201411
Text Language: English
Publisher: Geological Society of America (GSA), Boulder, CO, United States
References: 43
Accession Number: 2014-105160
Categories: Extraterrestrial geology
Document Type: Serial
Bibliographic Level: Analytic
Annotation: GSA Data Repository item 2014335
Illustration Description: illus.
Country of Publication: United States
Secondary Affiliation: GeoRef, Copyright 2017, American Geosciences Institute. Reference includes data from GeoScienceWorld, Alexandria, VA, United States. Reference includes data supplied by the Geological Society of America, Boulder, CO, United States
Update Code: 201452
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